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S. A. Lamb, N. C. Hearn, J. P. Morgan (University of Illinois), J. C. McDowell (Harvard-Smithsonian, CfA)
Current N-body/SPH simulations of collisions between two co-rotating disk galaxies indicate that objects with a morphology similar to that of Arp 220 can be produced rapidly, on timescales of order 100 million years, if the impact velocity is roughly parallel to the galactic spin axes. The simulations predict that extensive structures will be formed in both the gas and stars, extending tens of kiloparsecs from the eventual joint nuclear region. These structures, and a tilted, rotating gaseous disk can be approximately associated with features observed in Arp 220. Our simulations provide predictions of the velocity structure, and we compare these and morphological results with observations at a variety of wavelengths, including Chandra X-ray observations. We acknowledge support from NASA SAODO 0-1166B and DOE LLNL B506657.
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